A new source type of Galactic Cosmic Rays V.G. Sinitsyna , V.Yu. - - PowerPoint PPT Presentation

V.G. Sinitsyna , V.Yu. Sinitsyna , Yu. I. Stozhkov

P.N. Lebedev Physical Institute, RAS

A new source type of Galactic Cosmic Rays

The first detection of TeV gamma-rays from Red Dwarfs

The present point of view on the sources of cosmic rays in Galaxy considers explosions of supernovae as sources of these particles up to energies of 1017 eV. However, the experimental data obtained with Pamela, Fermi, AMS-02, spectrometers requires the existence of nearby sources of cosmic rays at the distances less then 1 kpc from the solar system. These sources could explain such experimental data as the growth of the ratio of galactic positrons to electrons with increase of their energy, the complex dependence of the exponent of the proton and alpha spectra from the energy of these particles, the appearance of anomaly component in cosmic rays. We consider active dwarf stars as possible sources of galactic cosmic rays in energy range up to 1014 eV. These stars produce powerful stellar flares. The generation of high-energy cosmic rays has to be accompanied by high-energy gamma-ray emission.

0.00 0.05 0.10 0.15 0.20 0.25 0.30 0.35 1 10 100 1000

e+ / (e- + e+) energy e , GeV

AMS-02 PAMELA calculation FERMI

Here we present the SHALON long-term observation data aimed to search for gamma-ray emission above 800 GeV from the active red dwarf stars. The data obtained during more than 10 years observations of the dwarf stars GL 851.1, V962 Tau, V780 Tau, V388 Cas and V1589 Cyg were analyzed. The high-energy gamma-ray emission in the TeV energy range mostly

• f flaring type from the sources mentioned above was detected. This result confirms that active dwarf stars are also the

sources of high-energy galactic cosmic rays (Stozhkov, 2011).

GCRs and ISM Interaction model

The first detection of TeV gamma-rays from Red Dwarfs

In the Galaxy, there are about 2×1011 stars. The dwarf stars belong to the G - M classes of the main sequence of stars, and they are in the bottom part of the right side of the Hertzsprung-Russel diagram. The number of such stellar objects is more than 90% of all stars in our

• Galaxy. These stars have temperatures T ≈ (2500 − 6000) K and mass

(0.06 − 1)M⊙, where M⊙ is the mass of our Sun. The luminosity of dwarf stars is in the range of (10−3 − 2)L⊙ where L⊙ is the solar luminosity, their radii are (0.1 − 1)R⊙ where R⊙ is the Sun radius. The nearest of the dwarf stars are at the distance of several parsecs from our solar system. It is believed that these stellar objects are uniformly distributed inside of the galactic disc (Gershberg, 1999, 2002). The stellar flares of active dwarf stars are sometimes taking place several times per day. The total energy release estimates as (1034 − 1036) erg (Gershberg, 1999, 2002; Maehara et al., 2012; Yang et al., 2017). The total energy of cosmic rays produced by the stellar flares of dwarf stars in the Galaxy is estimated as ~ WCR ≈ 1051 - 1053 ergs. This could provide the amount of energy of charged cosmic rays in our Galaxy even compared with ones provide by SN explosions. The consideration of active dwarf stars as sources of the cosmic rays with E ≤ 1014 eV are giving us the possibility to understand anomalies in the cosmic rays recorded during the last 10 - 15 years by PAMELA, AMS-02, CALET, DAMPE. These anomalies include the hardening observed in the spectra of cosmic ray nuclei at a rigidity of ∼ 300 GV, the different slopes of the proton and helium spectra (Adriani et al., 2011; Aguilar et al., 2015a,b), the rise in the positron fraction at particle energies above ∼ 8 GeV (Adriani et al., 2009; Aguilar et al., 2013) and others.

• Here we study the active dwarf stars that produce

powerful stellar flares and may accelerate cosmic-ray species up to 1014eV. Generation of high-energy cosmic rays in such flares should be accompanied by the high-energy γ -ray emission. We have used our SHALON instrument to detect the high-energy γ -rays in TeV-energy range.

• SHALON

are the imaging atmospheric Cherenkov telescopes creating in the P.N.Lebedev Physical Institute for gamma-ray astronomy at the energies of 800 GeV to 100

• TeV. The idea of enhancement of angular

resolution and sensitivity to the γ-rays with construction of the wide field of view was realized in SHALON telescopes since the construction.

• SHALON experiment aimed on 800 GeV – 100

TeV gamma-astronomy has been successfully

• perating

since 1992 and covers the wide astroparticle physics topics including an acceleration and

• rigin
• f

cosmic rays in supernova remnants, the physics of relativistic flaring objects like a black holes and active galactic nuclei as well as the long-term studies of the different type objects.

Detection of TeV gamma-rays from active dwarf stars

SHALON-2 SHALON-1

SHALON-1 SHALON-2

• The size of the composed spherical mirror - 11.2 m2
• A mirror is composed of 38 spherical mirrors of 60 cm

in diameter

• The mirror's radius of curvature is

R =8.5 m

• The angles of the mirror's turn

azimutal - 0° - З60°; zenith - 0° - 110°

SHALON-2 SHALON-1

SHALON OBSERVATORY for 800 GeV – 100 TeV gamma-astronomy

• Accuracy of guidance of the telescope central axis <0.1°
• Distance between the mirrors and the lightreceiver

F = 0.47 R = 4.1 m

• Field of view

> 8о

• Altazimuth mounting
• Parallactic mounting
• The mirror's weight - ~1 ton
• The weight of the lightreceiver 200 kg
• Total weight - 6 ton

SHALON mirror Cherenkov telescope created in 1992

SHALON-2 SHALON-1

The idea of enhancement of angular resolution and sensitivity to the γ-rays with construction of the wide field of view was realized in SHALON telescopes since the construction in 1992

• The distance between the mirror and the lightreceiver

F=0,47R=4.1m

• Number of photomultipliers

144(12х12)

• Type of photomultipliers

FEU-85 (PMT-85)

• The telescope's field of view

>8°

>8°

SHALON OBSERVATORY for 800 GeV – 100 TeV gamma-astronomy

Metal square-cone lightguide is used to improve light collection

FEU-85

Sinitsyna, Int. Workshop VHE Gamma Ray Astronomy Crimia, (1989)

The performance

• f

Cherenkov telescope together with selection criteria is summarized by its angular resolution and gamma-ray flux sensitivity. The accuracy of the determination of the coordinates of the γ- ray shower source in SHALON is ~0.07о (Sinitsyna 2014) and it is

SHALON-2 SHALON-1

SHALON OBSERVATORY for 800 GeV – 100 TeV gamma-astronomy

The sensitivity of the telescope is defined as the flux for 50 h of

• bservation of a point-like source at a

confidence level of 5σ (according to the formulation of Li&Ma). The SHALON minimum detectable integral flux of γ-rays at energy of 1 TeV is 2.1×10-13 cm-2 s-1. In the region 1–50 TeV the minimum detectable flux falls down to the value

• f

6×10-13 cm-2 s-1 and then, at energies E > 50 TeV, it grows because

• f limited telescopic field of view

(Sinitsyna et al. Adv.Sp.R 2017, Sinitsyna Astr.Lett, 2018).

increased by a factor of ~10 after additional processing (Sinitsyna Astr.Lett

2014, 2018). Sensitivity of γ-ray telescopes and detectors at 100 GeV – 100TeV.

• Plerions
• Shell-type SNRs
• Flaring stars
• Binaries
• Seyfert Galaxies
• Radio Galaxies
• Blazars
• Flat spectrum radio-

quazars

SHALON OBSERVATORY for 800 GeV – 100 TeV gamma-astronomy

Operated since 1992

The flare frequency of the active red dwarf stars is uncertain, and their

• bservations

require a long-term monitoring program. In accordance with the long-term program of observations of the Galactic γ -ray sources, more than ten- years long observations of the Tycho’s SNR, Crab Nebula, and Cyg X-3 have been carried out by the SHALON experiment.

SHALON telescope field of view during the

• bservation of Tycho’s SNR

V388 Cas

During the observations of Tycho’s SNR the SHALON field of view contains V388 Cas as it located at ~4.5o South from Tycho’s SNR . So due to the large telescopic field of view (~8o) the

• bservations
• f

Tycho’s SNR is naturally followed by the observations of V388 Cas flaring star. V388 Cas as a source accompanying to Tycho’s SNR was observed with SHALON telescope at the period 1996y to 2010y for a total of 93 hours. The γ-ray source associated with the V388 Cas was detected above 1 TeV with a statistical significance 6.8σ determined by Li&Ma and with average gamma-ray flux: IV388Cas(>1TeV) = (0, 840,19)•10-12 cm-2s-1

During long-term observation V388 Cas appeared as a source with variating flux and seemed to be detected during the flares.

V388 Cas as a source accompanying to Tycho’s SNR have been systematically observed with SHALON telescope during the clear moonless nights at zenith angles from 16o to 35o. The observations were performed using the standard for SHALON technique of recording information about the cosmic-ray background and gamma-ray-initiated showers in the same observing session. With the data processing, V388 Cas was detected above 0.8 TeV by SHALON with a statistical significance 6.8σ determined by Li&Ma

• method. The signal significance for this source is much less then
• ne for the source with similar flux and spectrum index obtained in

the same observation hours because of less collection field of view relative to the standard procedure of SHALON experiment. After the procession of the Tycho’s SNR observation data first by selection criteria associated with Tycho’s SNR and then with V388 Cas we found that less 1% of showers are common for the both

• sources. Recognition of source of each of the common showers is

performed by the analysis of angular distance of arrival direction of these showers and source coordinates. This didn’t change the average flux of Tycho’s SNR.

The -ray spectra of V388 Cas by SHALON Emission map of V388 Cas by SHALON

The shape of SHALON average differential spectrum of gamma rays from V388 Cas in the energy range from 0.8 to 25 TeV fits well to a soft power law : dN/dE=(0,910,22)×10-12×(Eγ./1 TeV)-2,520,15

with the 2/Dof= 1,23 where degree of freedom Dof = 6

A flaring spectrum: dN/dEFlare=(2,70,15)×10-12×(Eγ./1 TeV)-2,910,18

V388 Cas

Searching for counterparts in the Fermi-LAT 8 years catalogue (FL8Y), we found an unassociated source J0106.4 + 5938 of high energy emission that is located at the distance of ∼ 2.5◦ from V388 Cas. The FL8Y source catalogue is based on the data taken during the period from 2008 August 4 to 2016 August 2. The emission from J0106.4 + 5938 was detected by Fermi LAT at the level of 4.2 σ significance in the energy range from 100 MeV to 1 TeV. Giving the large distance to V388 Cas this object can’t be associated with this red dwarf.

The -ray spectra of V388 Cas by SHALON. The grey bow tie on V388 Cas plot indicates the minimum flux needed for a Fermi LAT 5 σ detection of a soft-spectrum point urce Emission map of V388 Cas by SHALON

There is an X-ray (0.1

• 2.4

keV) source, 2RXS°010318.3+622140, in the second ROSAT catalogue (Boller et al., 2016) located 15.3’’ away from the V388 Cas

• bject, with a quoted position uncertainty of 18’’.

The X-ray flux is 1.53×10−12erg cm−2s−1 and photon index −1.95±0.6 of simple power-law fit. It is also found in the first ROSAT catalogue.

V388 Cas

2RXS°010318.3+622140

V780 Tau and V962 Tau flaring stars are in the telescopic field of view during observations of Crab Nebula. V780 Tau is located at the distance of ~3о north from Crab and V962 Tau is

• f 2.5о east from Crab. As a result,

V780 Tau and V962 Tau as a sources accompanying to Crab have been systematically

• bserved

with SHALON telescope since 1994 during the clear moonless nights.

SHALON telescope field of view during the

• bservation of Crab Nebula

V780 Tau and V962 Tau

These flaring stars as a source accompanying to Crab were observed with SHALON telescope at the period 1994y to 2014y for a total of 125.2 hours during the clear moonless nights at zenith angles from 15o to 35o. The observations were performed using the standard for SHALON technique of recording information about the cosmic-ray background and gamma- ray-initiated showers in the same observing session. With the data processing, V780 Tau and V962 Tau were detected above 0.8 TeV by SHALON with the average integral flux : IV780Tau(>1TeV) = (0,230,03)•10-12 cm-2s-1 IV962Tau(>1TeV) = (0,390,04)•10-12 cm-2s-1

V780 Tau was detected above 0.8 TeV by SHALON with a statistical significance 6,1σ determined by Li&Ma method. The signal significance for this source is also much less then one for the source with similar flux obtained in the same observation hours because of less collection field of view relative to the standard experiment procedure. After the procession of the Crab

• bservation data first by selection criteria associated with Crab

and then with V780 Tau we found that less than 1% of showers are common for the both sources. Recognition of source of each

• f the common showers is performed by the analysis of angular

distance of arrival direction of these showers and source

• coordinates. As a result, less than ~ 0,4% of Crab showers were

recognized to be V780 Tau showers. This didn’t change the average flux of Crab. In observations since 1994y V780 Tau was fount to be variating. The flaring spectrum was also extracting ().

V780 Tau

The shape of SHALON differential spectrum of gamma rays from V780 Tau in the energy range from 0.8 to 20 TeV fits well to a soft power law: dN/dE=(0,210,08)×10-12×(Eγ./1 TeV)-2,510,15

with the 2/Dof= 1,31 where degree of freedom Dof = 5

A flaring spectrum: dN/dEFlare=(2,00,15)×10-12×(Eγ./1TeV)-3,010,21

Emission map of V780 Tau by SHALON The -ray spectra of V780 Tau by SHALON

An unassociated object FL8Y J0540.5 + 2305 is located at a distance of ∼ 1.6◦ from V780 Tau. The emission from the unassociated source was detected by Fermi LAT at the level of 6.62 σ significance in the energy range from 100 MeV to 1 TeV. Giving the large distance to V780 Tau this object can’t be associated with this red dwarf. In observations since 1994y V780 Tau was fount to be variating. The flaring spectrum was also extracting (). The luminosity of V962 Tau during the high flux periods lasting of 4 days is ∼ 1.2×1029 erg s−1 (assuming the distance of 10pc) and its integrated radiated energy ∼ 2.5×1034ergs. The average non- flaring luminosity is ∼ 1 × 1028erg s−1.

V780 Tau

The counterpart of V780 Tau in the ROSAT second catalogue (Boller et al., 2016) is 2RXS J054025.1 + 244839 object. It located in 25’’ from the red dwarf star with a position uncertainty of 26’’. Its X-ray flux is 3.6 × 10−13erg cm−2s−1.

Emission map of V780 Tau by SHALON The -ray spectra of V780 Tau by SHALON. The grey bow tie on V780 Tau plot indicates the minimum flux needed for a Fermi LAT 5σ detection of a soft-spectrum point

2RXS J054025.1 + 244839

V962 Tau

The differential spectrum of gamma rays from V962 Tau in the energy range from 0.8 to 20 TeV fits well to a soft power law : dN/dE=(0,400,17)×10-12×(Eγ./1 TeV)-2,540,15

with the 2/Dof= 0,87 where degree of freedom Dof = 6

A flaring spectrum: dN/dEFlare=(2,80,45)×10-12×(Eγ./1TeV)-2,950,22

V962 Tau was detected above 0.8 TeV by SHALON with a statistical significance 7,7σ determined by Li&Ma method. The signal significance for this source is also less then one for the source with similar flux obtained in the same

• bservation hours because of less collection field of view

relative to the standard experiment procedure. After the procession of the Crab observation data first by selection criteria associated with Crab and then with V780 Tau we found that there are no showers common for the both sources.

V962 Tau was also fount to be variating. The flaring spectrum is presented with . The luminosity of V962 Tau during the high flux periods lasting of 4 days is ∼ 1.2×1029erg s−1 (assuming the distance

• f 10pc) and its integrated radiated energy ∼ 2.5× 1034ergs.

The average non-flaring luminosity is ∼ 1×1028erg s−1.

Emission map of V962 Tau by SHALON The -ray spectra of V962 Tau by SHALON

V962 Tau

There is an X-ray source, 2RXS J054552.1 + 225248, located 3.7’’ away from the V962 Tau object, with a quoted position uncertainty

• f 10’’. The X-ray flux is 2.5 × 10−12erg cm−2s−1 and photon index

−1.92±0.8 of simple power law fit. It is also found in the first ROSAT catalogue. The emission from unassociated source 3FGL J0544.7 + 2239 (Acero et al., 2015) at the distance of ∼ 0.33◦ from V962 Tau was detected by Fermi LAT in the energy range 100 MeV - 300 GeV with significance of 4.24 σ . The Fermi-LAT spectrum was fitted with a power law dN / dE = C × (E / 1.26 GeV) − Γ, where Γ = 2.49 ± 0.18 and C = (5.1 ± 1.1) × 10−13MeV−1cm−2s−1. The Fermi-LAT spectrum of this unassociated source is consistent with the SHALON spectrum of V962 Tau at TeV energies. V962 Tau was also fount to be variating. The flaring spectrum is presented with . The luminosity of V962 Tau during the high flux periods lasting of 4 days is ∼ 1.2×1029erg s−1 (assuming the distance of 10pc) and its integrated radiated energy ∼ 2.5× 1034ergs. The average non-flaring luminosity is ∼ 1×1028erg s−1.

Emission map of V962 Tau by SHALON The SED of V962 Tau by SHALON and of the 3FGL J0544.7+2239 is shown with a bow tie

2RXS J054552.1 + 225248

V1589 Cyg is located at the distance

• f ~2о west from Cyg X-3. So due to

the large telescopic field of view >8o the observations of Cygnus-X are naturally followed by the tracing of V1589 Cyg. As a result, V1589 Cyg as a source accompanying to Cyg X-3 have been systematically observed with SHALON telescope (since 1995 up to 2016) during the clear moonless nights at zenith angles from 5o to 34o for a total of 303.5 hours .

SHALON telescope field of view during the

• bservation of Cyg X-3

V1589 Cyg

In accordance with the program on long-term studies of microquasar Cygnus X-3 at very high energies, observations of Cygnus Region and its objects, including V1589 Cyg, as well as TeV J2032+4130 and γCygni SNR are being carried out with SHALON. With the data processing, V1589 Cyg was detected above 0.8 TeV by SHALON with the average integral flux : IV1589Cyg(>0,8TeV) = (0,130,019)•10-12 cm-2s-1

V1589 Cyg as a source accompanying to Cyg X-3 have been systematically observed with SHALON. The observations were performed using the standard for SHALON technique of recording information about the cosmic-ray background and gamma-ray-initiated showers in the same observing session. With the data processing, V1589 Cyg was detected above 0.8 TeV by SHALON with a statistical significance 6.5σ determined by Li&Ma method. The signal significance for this source is less then one for the source with similar flux and spectrum index obtained in the same observation hours because of less collection field of view relative to the standard procedure of SHALON experiment. The corrections for the effective field of view were made. After the procession of the Cyg X-3

• bservation data first by selection criteria associated with Cyg X-3 and

then with V1589 Cyg we found that less than 2% of showers are common for the both sources. Recognition of source of each of the common showers is performed by the analysis of angular distance of arrival direction of these showers and source coordinates. As a result, less than 1% of Cyg X-3 showers were recognized to be V1589 Cyg

• showers. This didn’t change the average flux of Cyg X-3. During long-

term observation V1589 Cyg appeared as a source with variating flux. The flaring spectrum was also extracting and presented with .

V1589 Cyg

The shape of SHALON differential spectrum of gamma-rays from V1589 Cyg in the energy range from 0.8 to 35 TeV fits well to a soft power law: dN/dE=(0,150,05)×10-13×(Eγ./1 TeV)-2,910,18

with the 2/Dof= 0,89 where degree of freedom Dof = 5 A flaring spectrum: dN/dEFlare=(1,70,45)×10-12×(Eγ./1TeV)-3,150,29 Emission map of V1589 Cyg by SHALON The -ray spectra of V1589 Cyg by SHALON

An unassociated object FL8Y J2041.2 + 41.76 detected by Fermi- LAT at a distance of ∼ 0.45◦ from V1589 Cyg. The high energy emission was detected at the level of 5.6σ significance. The differential photon spectrum was obtained in the energy range from 100 MeV to 100 GeV. The spectrum was fitted with a power law dN/dE = C × (E / 1.63 GeV)− Γ, where Γ = 2.82 ±0.26 and C=(7.63 ± 1.3)×10−13MeV−1cm−2s−1. The FL8Y spectrum of J2041.2 + 41.76 is consistent with SHALON observations of V1589 Cyg at TeV energies. The duration of high flux periods (corresponding to the flare spectra by SHALON) for the V1589 Cyg is from 2 to 4 days, so the estimated luminosity is ∼ 8.5×1029erg s−1 (at ∼ 30 pc) and radiated energy ∼ 2.5×1035erg (average non-flaring luminosity of ∼6×1028erg s−1).

V1589 Cyg

The object 2RXS J204249.0 + 412246 from X-ray the ROSAT catalogue (Boller et al., 2016) located 14.4’’ from the V1589 Cyg, with a position uncertainty of 12’’. The X-ray flux is 8.49×10−13erg cm−2s−1 and simple power-law fit photon index of −2.16 ± 1.4. It has a counterpart in the first ROSAT catalogue.

Emission map of V1589 Cyg by SHALON The SED of V1589 Cyg by SHALON and the FL8Y J2041.2 + 41.76 is shown with a bow tie

2RXS J204249.0 + 412246

GL 851.1 is located at the distance of ~1.8о north from 4C+31.63. The observations of 4C+31.63 FSRQ type object was started in 2012 with SHALON in the framework of FSRQ studies at TeV energies which include the objects from the first and second Fermi LAT AGN catalogues. The

• bservations of 4C + 31.63 also include of

GL 851.1 dwarf star. The spectral class of GL 851.1 differs from one for objects presented above. It is a star of spectral class K (dK5V). It was also classified as a dM0e and located at the distance of 21.7 pc

SHALON telescope field of view during the

• bservation of 4C+31.63

GL 851.1

As a result, GL 851.1 as a source accompanying to 4C+31.63 have been systematically

• bserved with SHALON telescope (since 2012 up to 2015) during the clear moonless nights at

zenith angles from 5o to 34o for a total of 45 hours . With the data processing, GL 851.1was detected above 0.8 TeV by SHALON with the average integral flux : IGL851.1(>0,8TeV) = (0,550,019)•10-12 cm-2s-1 GL 851.1 3c+31.63

GL 851.1 was detected by SHALON above 0.8 TeV with statistical significance of 5.1 σ. Here we find that there are no showers common for the 4C + 31.63 and GL 851.1. The differential spectrum of γ -ray emission from GL 851.1 in the energy range from 0.8 to 10 TeV can be fitted with a power law: dN/dE = (0.52 ± 0.17)×10−12×(Eγ/1 TeV)−2.54±0.42 TeV−1cm−2s−1 with the χ2 / Dof = 0.91, where Dof = 4. The flaring spectrum is dN/dEFlare=(1.60±0.45)×10−12×(Eγ/1TeV)−2.32±0.21TeV−1cm−2s−1 GL 851.1 shows the flaring period with the duration of 5 days and corresponding estimated luminosity is 7.8×1029erg s−1 (at 21.7 pc); integrated radiated energy for the high period ∼ 3.4 × 1035ergs. (average non-flaring luminosity of ∼ 2× 1029erg s−1).

GL 851.1

The emission from unassociated source FL8Y J2210.9 + 3202 at the distance of ∼ 0.5◦ from GL 851.1 was detected by Fermi LAT in the energy range 100 MeV – 1 TeV with significance of 5.29 σ. The Fermi-LAT spectrum was fitted with a power law dN/dE = C×(E/ 9.99 GeV)−Γ , where Γ = 1.73 ± 0.20 and C = (1.52 ± 0.44) × 10−15 MeV−1cm−2s−1. The Fermi-LAT spectrum

• f this unassociated source is consistent with the SHALON

spectrum of GL 851.1 at TeV energies.

The SED of GL 851.1 by SHALON and the FL8Y J2210.9 + 3202 is shown with a bow tie The -ray spectra of GL 851.1 Cyg by SHALON

It was show in the studies of flaring stars that the frequency of flaring is uncertain, so for the searching for TeV gamma-ray emission from these objects we choose objects we have collected data from different long-term

• bservations.

Light curves of GL 851.1, V388 Cas, V780Tau, V962 Tau and V1589 Cyg

The light curves of GL 851.1, V388 Cas, V780Tau, V962 Tau and V1589 Cyg at TeV energies

• btained

in the long-term SHALON observations. The integral fluxes averaged over the each year observation period are shown. During long-term

• bservations, red dwarfs appeared

as sources with variating flux and seemed to be detected during the flares (especially V388 Cas and GL 851.1).

GL 851.1 shows the flaring period with the duration

• f 5 days and corresponding estimated luminosity is

7.8×1029erg s−1 (at 21.7pc); integrated radiated energy for the high period ∼ 3.4×1035 ergs. (average non- flaring luminosity of ∼ 2 × 1029erg s−1). V388 Cas has been detected during the flares that

• ccurred before 2008. It was found that the duration
• f high flux periods for the V388 Cas is four days.

The estimated luminosity (at 10.5pc) corresponding to high periods is ∼ 1.5 × 1029 erg s−1 and its integrated radiated energy ∼ 5.1 × 1034 erg. The average non- flaring luminosity is of ∼ 6.5 × 1028erg s−1. The luminosity of V962 Tau during the high flux periods lasting of 4 days is ∼ 1.2×1029 erg s−1 (assuming the distance of 10pc) and its integrated radiated energy ∼ 2.5×1034ergs. The average non- flaring luminosity is ∼ 1 × 1028erg s−1. The luminosity of V962 Tau during the high flux periods lasting of 4 days is ∼ 1.2×1029 erg s−1 (assuming the distance of 10pc) and its integrated radiated energy ∼ 2.5×1034ergs. The average non- flaring luminosity is ∼ 1 × 1028erg s−1. The duration of high flux periods for the V1589 Cyg is from 2 to 4 days, so the estimated luminosity is ∼ 8.5×1029erg s−1 (at ∼ 30 pc) and radiated energy ∼ 2.5×1035erg (average non-flaring luminosity

• f

∼6×1028erg s−1).

Light curves of GL 851.1, V388 Cas, V780Tau, V962 Tau and V1589 Cyg

M-Dwarf stars are characterized by flaring events which occur frequently with flare duration varies. It was found that the duration

• f high flux periods corresponding to the flare spectra for the red

dwarfs discussed above ranges from 2 to 5 days. Very high energy γ-ray fluxes found here demonstrate that these objects produce the flares of ~1034–1035ergs. The energy released in a stellar flares and its frequency are able to provide the necessary energy of GCRs in the disk of our Galaxy and make a significant contribution to the GCR spectrum up to energies of Е≈ 1013-1014 eV (Stozhkov, 2011). The urgent point is that the sources of GCRs are placed at the distances less then 1 kpc from the solar system. Then some of these accelerated GCR escape into the interstellar medium and then interact. An source of positrons is the decay of neutral pions into two γ-rays and the subsequent formation of е+ е– pairs by these gamma rays.

GCRs from M-Dwarf star flares

Positrons and electrons from stellar flares with Е > 5 GeV escape into the interstellar medium from a flare region with strong magnetic fields. Thus, there is an additional source of е+ that explains the anomalous PAMELA effect. It should be noted that most of the electrons (and protons) are accelerated during the stellar flare and the addition of another е– flux via the mechanisms of π° and π– decays constitutes only a small part of the main flux. The additional source of е+, however, provides the main flux of these particles in the Galaxy up to energies of Е ≈ (300–400) GeV.

(see Stozhkov, Bull. RAS, 75(3), p323, 2011 and Sinitsyna, Sinitsyna, Stozhkov, ASR 2019 doi.org/10.1016/j.asr.2019.08.024

). e+ Excess calculations due to Dwarf star flares (Stozhkov, 2011)

PAMELA positron data

M-Dwarf stars are characterized by flaring events which occur frequently with flare duration varies in time but total duration of >104s. Very high energy γ-ray fluxes presented here demonstrate that these objects produce the flares of ~1034– 1035ergs. The energy released in a stellar flares and its frequency are able to provide the necessary energy of GCRs in the disk of our Galaxy and make a significant contribution to the GCR spectrum up to energies of Е≈1013–1014 eV (Stozhkov, 2011). The urgent point is that the sources of GCRs are placed at the distances less than 1 kpc from the solar system. Then some of these accelerated GCR escape into the interstellar medium and then interact. An source

• f positrons is the decay of neutral pions into two gamma-rays

and the subsequent formation of е+ е– pairs by these gamma rays.

GCRs from M-Dwarf star flares

Positrons and electrons from stellar flares with Е > 5 GeV escape into the interstellar medium from a flare region with strong magnetic fields. Thus, there is an additional source of е+ that explains the anomalous PAMELA effect. It should be noted that most of the electrons (and protons) are accelerated during the stellar flare and the addition of another е– flux via the mechanisms of π° and π– decays constitutes only a small part of the main flux. The additional source of е+, however, provides the main flux of these particles in the Galaxy up to energies of Е ≈ (300–400) GeV. But, above 350 GeV according to the scenario suggested in (Stozhkov, 2011) the positron fraction has to decrease to the values calculated in because the highest energy of accelerated particles in the stellar flares is unlikely to exceed 1013eV e+ Excess calculations due to Dwarf star flares (Stozhkov, 2011)

PAMELA and AMS positron data

(Moskalenko&Strong, 1998)

Red stars of Flare star cataloguea,b viewed by SHALON

2RXS J204249.0+412246

FL8Y J2210.9 + 3202 FL8Y J2041.2 + 41.76

2RXS J054552.1 + 225248

3FGL J0544.7 + 2239

2RXS J054025.1 + 244839 2RXS 010318.3+622140

ROSAT (0.1 - 2.4 keV) Fermi LAT (>100 MeV)

Sinitsyna, Sinitsyna, Stozhkov ASR 2019 doi.org/10.1016/j.asr.2019.08.024